Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817
One unanswered question about the binary neutron star coalescence GW170817 is the nature of its post-merger remnant. A previous search for post-merger gravitational waves targeted high-frequency signals from a possible neutron star remnant with a maximum signal duration of 500 s. Here, we revisit th...
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| Published in | The Astrophysical journal Vol. 875; no. 2; pp. 160 - 178 |
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| Main Authors | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
| Format | Journal Article |
| Language | English |
| Published |
Philadelphia
The American Astronomical Society
20.04.2019
IOP Publishing American Astronomical Society University of Chicago Press |
| Subjects | |
| Online Access | Get full text |
| ISSN | 0004-637X 1538-4357 1538-4357 |
| DOI | 10.3847/1538-4357/ab0f3d |
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| Abstract | One unanswered question about the binary neutron star coalescence GW170817 is the nature of its post-merger remnant. A previous search for post-merger gravitational waves targeted high-frequency signals from a possible neutron star remnant with a maximum signal duration of 500 s. Here, we revisit the neutron star remnant scenario and focus on longer signal durations, up until the end of the second Advanced LIGO-Virgo observing run, which was 8.5 days after the coalescence of GW170817. The main physical scenario for this emission is the power-law spindown of a massive magnetar-like remnant. We use four independent search algorithms with varying degrees of restrictiveness on the signal waveform and different ways of dealing with noise artefacts. In agreement with theoretical estimates, we find no significant signal candidates. Through simulated signals, we quantify that with the current detector sensitivity, nowhere in the studied parameter space are we sensitive to a signal from more than 1 Mpc away, compared to the actual distance of 40 Mpc. However, this study serves as a prototype for post-merger analyses in future observing runs with expected higher sensitivity. |
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| AbstractList | One unanswered question about the binary neutron star coalescence GW170817 is the nature of its post-merger remnant. A previous search for post-merger gravitational waves targeted high-frequency signals from a possible neutron star remnant with a maximum signal duration of 500 s. Here, we revisit the neutron star remnant scenario and focus on longer signal durations, up until the end of the second Advanced LIGO-Virgo observing run, which was 8.5 days after the coalescence of GW170817. The main physical scenario for this emission is the power-law spindown of a massive magnetar-like remnant. We use four independent search algorithms with varying degrees of restrictiveness on the signal waveform and different ways of dealing with noise artefacts. In agreement with theoretical estimates, we find no significant signal candidates. Through simulated signals, we quantify that with the current detector sensitivity, nowhere in the studied parameter space are we sensitive to a signal from more than 1 Mpc away, compared to the actual distance of 40 Mpc. However, this study serves as a prototype for post-merger analyses in future observing runs with expected higher sensitivity. One unanswered question about the binary neutron star coalescence GW170817 is the nature of its post-merger remnant. A previous search for post-merger gravitational waves targeted high-frequency signals from a possible neutron star remnant with a maximum signal duration of 500 s. Here we revisit the neutron star remnant scenario with a focus on longer signal durations up until the end of the Second Advanced LIGO-Virgo Observing run, 8.5 days after the coalescence of GW170817. The main physical scenario for such emission is the power-law spindown of a massive magnetar-like remnant. We use four independent search algorithms with varying degrees of restrictiveness on the signal waveformand different ways of dealing with noise artefacts. In agreement with theoretical estimates, we find no significant signal candidates. Through simulated signals, we quantify that with the current detector sensitivity, nowhere in the studied parameter space are we sensitive to a signal from more than 1 Mpc away, compared to the actual distance of 40 Mpc. This study however serves as a prototype for post-merger analyses in future observing runs with expected higher sensitivity. |
| Author | Flaminio, R. Caride, S. Arène, M. Shah, A. A. Cagnoli, G. Pinto, I. M. Bozzi, A. Ward, R. L. Brisson, V. Crowder, S. G. Sutton, P. J. Essick, R. C. Junker, J. Heptonstall, A. W. Pedersen, C. Leavey, S. Pang, B. Nolting, D. Booth, C. D. Feng, F. Koley, S. Holz, D. E. Souradeep, T. Robinet, F. Khan, S. Muñiz, E. A. Wittel, H. Martin, I. W. Pedraza, M. Torres-Forné, A. Garcia, A. Hanna, C. Worden, J. Smith, B. McCarthy, R. Cerretani, G. Danilishin, S. L. Corban, P. Favata, M. Cunningham, L. Kim, K. Ananyeva, A. Boer, M. Pankow, C. Bossie, K. Font, J. A. Hinderer, T. Tacca, M. Nitz, A. Fong, H. Coughlin, S. B. Chung, S. Lockerbie, N. A. Wade, M. Davier, M. Dmitriev, A. Prodi, G. A. Lehmann, J. Pitkin, M. Pratt, J. W. W. Verkindt, D. Miller, A. L. Passaquieti, R. Chatterjee, D. Wang, Y. F. Kim, J. C. Frasconi, F. Yvert, M. Beer, C. Thomas, E. G. Gushwa, K. E. Gaudio, S. Zhang, T. De Pietri, R. Strigin, S. E. Cannon, K. C. Denker, T. Raab, F. J. Salemi, F. Oh, S. H. Tsuna, D. Dattilo, V. Naticchioni, L. Weinstein, A. J. Pai, S. A. Zendri, J.-P. Kang, G. Constancio, M. Cleva, F. |
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| Copyright | 2019. The American Astronomical Society. All rights reserved. Copyright IOP Publishing Apr 20, 2019 Attribution |
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| Snippet | One unanswered question about the binary neutron star coalescence GW170817 is the nature of its post-merger remnant. A previous search for post-merger... |
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| SubjectTerms | Algorithms Astrophysics Aérospatiale, astronomie & astrophysique Binary stars Coalescence Coalescing Computer simulation General Relativity and Quantum Cosmology Gravitational waves Magnetars methods: data analysis Neutron stars Neutrons Parameter sensitivity Physical, chemical, mathematical & earth Sciences Physics Physique, chimie, mathématiques & sciences de la terre Power law Search algorithms Sensitivity analysis Space science, astronomy & astrophysics Star mergers Stars & galaxies stars: neutron Waveforms |
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| Title | Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817 |
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